1. EGOs: Massive YSOs in IRDCs Ed Churchwell & Claudia Cyganowski with co-workers: Crystal Brogan, Todd Hunter, Barb Whitney Qizhou Zhang Dense Cores in Dark Clouds LXV Oct. 21-22, 2009

2. The Evolution of IR-selected MYSOs (which occur in Dense and Massive Cores) IRASMSXSpitzer (IRAC) Cyganowski et al. 2008 RGB: 100, 25, 12  m Resolution ~ 0.5’-2’ RGB: 21.4, 12.1, 8.3  m Resolution ~ 18” RGB: 8.0, 4.5, 3.6  m Resolution ~ 2”

3. Image: NASA/JPL -CalTech Reach et al (2006) Spitzer, 3.6um- 24um (with <6” resolution) A New Diagnostic: Spitzer’s 4.5  m band

4. A New MYSO Outflow Sample: Extended Green Objects (EGOS) from GLIMPSE Cyganowski et al. (2008) Red: 8.0um, Green: 4.5um, Blue: 3.6um

7. SEDs of two typical EGOs

8. EGOs: Infrared Properties Cyganowski et al. (2008) Number of EGOs Separation from nearest IRAS PS (arcmin) Stage I Stage II Stage III Average separation between an EGO and nearest IRAS point source ≤2’ MIR colors of EGOs are consistent with young protostars still embedded in infalling envelopes > 300 EGOs in GLIMPSEI survey area

9. EGOs: Found in Molecular Cloud Cores CO Cyganowski et al. (2008) EGO positions overplotted on integrated CO emission (contours) from Dame et al. (2001).

10. EGOs also located toward IRDCs note images

11. EGOs: Correlation with 6.7 GHz Class II CH 3 OH masers from the literature Separation from maser (arcseconds) Number of EGOs Cyganowski et al. (2008) Correlation analysis based on published surveys requires: (1) maser positions known to <1” and (2) maser surveys with well-defined coverage Of EGOs in areas of published surveys, 47% associated with 6.7 GHz masers But, coverage limited and sensitivity uneven: dedicated maser searches towards EGOs required 6.7 GHz Class II CH 3 OH masers are associated exclusively with massive YSOs (e.g. Minier et al. 2003)

12. Are EGOs Massive YSOs with Outflows? Image courtesy of NRAO/AUI Observational Tests: High-resolution (E)VLA survey for 6.7 GHz CH 3 OH masers (associated exclusively with massive YSOs, Minier et al. 2003) High-resolution VLA survey for 44 GHz CH 3 OH masers (associated with molecular outflows, Kurtz et al 2004) Single-dish (JCMT) surveys for SiO, HCO +, H 13 CO +, thermal CH 3 OH emission Sample of ~28 EGOs, selected to: Cover range of MIR properties (8/24um counterparts, morphology, angular extent of 4.5um emission) Be visible from northern hemisphere

13. Cyganowski et al. 2009 Images: Red: 8um, Green: 4.5um, Blue: 3.6um (GLIMPSE). Yellow contours: MIPS 24 um Magenta Crosses: 44 GHz Class I CH 3 OH masers. Black Diamonds: 6.7 GHz Class II CH 3 OH masers EGO Survey Results: Spatial Distribution of CH 3 OH Masers

14. Cyganowski et al. 2009 Profiles: Dotted: HCO + (3-2) Solid: H 13 CO + (3-2) Dashed: 6.7 GHz CH 3 OH maser (scaled) Diamonds show velocity range spanned by 44 GHz CH 3 OH maser emission EGO Survey Results: Kinematics of CH 3 OH Maser and Thermal Molecular Line Emission

15. EGO Survey Results: CH 3 OH Maser Kinematics Left: Grayscale: 4.5  m (GLIMPSE). X: 44 GHz CH 3 OH masers, color-coded by velocity. The black rectangle is the field of view shown at right. Right: Fitted positions, with errors, of 6.7 GHz CH 3 OH masers, color-coded by velocity. Fitted positions with errors >0.15” (S/N<10) are not shown, those with errors between 0.05” and 0.15” (10<S/N<30) are shown as light lines. The bin color-coded green is approximately centered on the gas v(LSR) of ~60 km/s. To increase the range of distinguishable colors, purple is used to represent the most blueshifted masers.

16. Image: Red: 8um, Green: 4.5um, Blue: 3.6um (GLIMPSE). Yellow contours: MIPS 24 um Magenta Crosses: 44 GHz Class I CH 3 OH masers. Black Diamonds: 6.7 GHz Class II CH 3 OH masers Cyganowski et al. 2009 EGO Survey Results: Methanol Masers and Thermal Line Emission ~0.18 pc SiO(5-4) G11.92-0.61

17. Next Steps: (Sub)mm Line and Continuum Observations Cyganowski et al., in prep. Images: Red: 8um, Green: 4.5um, Blue: 3.6um (GLIMPSE). Contours: 1.3 mm continuum emission (black) and high velocity 12 CO(2-1) emission from the SMA. (a) The EGO G11.92-0.61. 12 CO (2-1) integrated over v~ -24 to 25 km/s (blue) and v~ 41-71 km/s (red). Though multiple compact cores are present, there is one dominant outflow. (b) The EGO G19.01-0.03. 12 CO (2-1) emission integrated over v~ -46 to 40 km/s (blue) and v~ 79-92 km/s (red); emission nearer the systemic velocity is dominated by an extended envelope, indicating that the source is very young. The SMA synthesized beam is shown at lower left in each panel (~3”~12000 AU at ~4 kpc).

18. EGO Survey Results: Summary 6.7 GHz CH 3 OH maser detection rate towards EGOs >64% Nearly double the detection rate of surveys using other MYSO selection criteria Centrally concentrated, coincident with 24µm emission 44 GHz CH 3 OH maser detection rate ~ 89% towards EGOs with 6.7 GHz masers Spatially distributed, coincident with 4.5µm emission HCO + (3-2) line profiles->broad vel widths (mostly infall) SiO (5-4) detection rate 90% -> recently shocked gas (outflows and/or infall) 95% nondetection rate for bright 44 GHz continuum emission-> most surveyed EGOs are not UC HII regions Bottom line: Surveyed EGOs are young MYSOs with active outflows, and hence presumably ongoing accretion

19. Cyganowski et al. 2009 G11.92-0.61 (SE source) Jy/beam mJy/beam km/s G19.01-0.03 C 2 H 5 CN HNCO CH 3 CN(J=12-11) Cyganowski et al., in prep. In 2 EGOs, both selected to have bipolar 4.5  m morphology, an associated 24  m source, and 6.7 and 44 GHz CH 3 OH masers: there is a single dominant bipolar molecular outflow, traced by 12 CO(2-1) and coincident with the 4.5  m lobes the driving source of the 4.5  m outflow is a compact mm core Diversity: One EGO is associated with a cluster of at least 3 compact cores, while the other appears to be a single MYSO (at the ~3” resolution of the SMA data) In G11.92, the driving source of the outflow is a hot core (upper left); other 2 mm cores are devoid of line emission G19.01 has weaker hot core signatures, CO emission near v(LSR) indicative of extended envelope (younger?) SMA Results (Preliminary)

20. Understanding EGOs: Next Steps Preliminary analysis of a small subsample of EGOs shows range of properties (SMA 1.3 mm observations) Need high resolution (sub)mm data for larger samples of EGOs (SMA, upcoming ALMA Early Science): Outflow kinematics Multiplicity, physical conditions, and masses of dense cores (possible driving sources) High resolution cm continuum observations to constrain presence and physical properties of ionized gas